Reducing Uncertainties in the Production of the Gamma-emitting Nuclei 26Al, 44Ti, and 60Fe in Core-collapse Supernovae by Using Effective Helium Burning Rates

Sam M. Austin1,2, Christopher West2,3,4, and Alexander Heger2,3,5,6
The Astrophysical Journal Letters 839 L9 Link to Article [https://doi.org/10.3847/2041-8213/aa68e7]
1National Superconducting Cyclotron Laboratory, Michigan State University, 640 South Shaw Lane, East Lansing, MI 48824-1321, USA
2Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824-1321, USA
3Minnesota Institute for Astronomy, School of Physics and Astronomy, University of Minnesota, Twin Cities, Minneapolis, MN 55455-0149, USA
4Center for Academic Excellence, Metropolitan State University, St. Paul, MN, 55106, USA
5Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, VIC 3800, Australia
6Center for Nuclear Astrophysics, Department of Physics and Astronomy, Shanghai Jiao-Tong University, Shanghai 200240, P. R. China

We have used effective reaction rates (ERRs) for the helium burning reactions to predict the yield of the gamma-emitting nuclei 26Al, 44Ti, and 60Fe in core-collapse supernovae (SNe). The variations in the predicted yields for values of the reaction rates allowed by the ERR are much smaller than obtained previously, and smaller than other uncertainties. A “filter” for SN nucleosynthesis yields based on pre-SN structure was used to estimate the effect of failed SNe on the initial mass function averaged yields; this substantially reduced the yields of all these isotopes, but the predicted yield ratio 60Fe/26Al was little affected. The robustness of this ratio is promising for comparison with data, but it is larger than observed in nature; possible causes for this discrepancy are discussed.

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